Planetary Formation and Evolution Revealed with a Saturn Entry Probe: The Importance of Noble Gases

The determination of Saturn’s atmospheric noble gas abundances are critical to understanding the formation and evolution of Saturn, and giant planets in general. These measurements can only be performed with an entry probe.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

We recommend that the Decadal Survey place a high priority on continued, even expanded, support of the Research & Analysis programs that fund the efforts of exoplanet theorists, laboratory workers, and observers through NASA’s and NSF''s research programs.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

The study of planetary ring systems forms a key component of planetary science. We discuss priority activities for the next decade including full support for the Cassini Solstice Mission, a spacecraft mission to Neptune and/or Uranus, and support for Earth-based research activities.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

We outline atmospheric science goals and requirements for Jupiter in the next decade exploration (Juno, EJSM, Observatories, probes) in 5 themes: formation and evolution, weather-layer dynamics, coupling with the interior, interactions with the external environment and time-variable phenomena.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

Neptune Ring Science with Argo - A Voyage through the Outer Solar System

Argo, an innovative concept for a New Frontiers 4 mission, will yield significant advances in our understanding of evolutionary processes of rings and small bodies in the outer Solar System by executing a flyby through the Neptune system, then going on to a scientifically-selected KBO.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

Earth-Based Observational Support for Spacecraft Exploration of Outer-Planet Atmospheres

This white paper advocates continued robust Earth-based observational support for spacecraft missions, addressing in particular investigations of Giant Planet atmospheres. Recommendations include upgrades to the NASA IRTF as well as cooperative investments in large or giant telescopes.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

This paper discusses some of the fundamental science that must be done at Uranus if we are to understand our Solar System and systems discovered around other stars. We suggest a Uranus Orbiter should be launched in the next decade.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

We believe many important atmospheric science questions can only be addressed by studies of the ice giants Uranus and Neptune. These questions relate to fundamental atmospheric processes that help us understand the formation, evolution, and current structure of all planets.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

Argo is an innovative pragmatic concept for a New Frontiers 4 mission which exploits an upcoming launch window that permits a close Triton encounter during a flyby through the Neptune system, and then continues on to a scientifically-selected Kuiper Belt Object.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

It is recommended that probe missions to the giant planets be performed to help constrain models of solar system formation and the origin and evolution of atmospheres, to provide a basis for comparative studies of the gas and ice giants, and to provide a valuable link to extrasolar planetary systems

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

This paper discusses the capability of heritage TPS technology used on the Galileo probe and new materials required for future outer planet probe missions. A prime conclusion is that there are important issues regarding the availability of the TPS required for Outer Planet entry probes.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

The purpose of this White Paper is to highlight areas of knowledge of our Solar System that will be important in interpreting future observations of exoplanets, especially giant exoplanets, and also how the diversity of exoplanets can inform our understanding of the Solar System.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

This is the final version of a white paper which provides the OPAG recommendations for technology required to undertake outer planetary missions. The paper describes the need for an OP technology program and provides specific recommendations for NASA investments during the next decade.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

The challenge associated with operating a spacecraft for long periods within the radiation belts of Jupiter cannot be underestimated. To realize the promise of incredible science the risk must be identified and controlled. Given the identified steps, the design is well in hand and would allow this s

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

The Europa Jupiter System Mission (EJSM) is guided by the overarching theme: the emergence of habitable worlds around gas giants, with goals to determine whether the Jupiter System harbors habitable worlds, and to characterize the processes within the Jupiter system.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

In this white paper I argue that Titan provides a strict test for the Copernican hypothesis that life is a ubiquitous cosmic phenomenon. Planets with environments like Titan may be common in the cosmos, as they correspond to a roughly 1 AU orbit around M-dwarfs.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Future Io Exploration for 2013-2022 and Beyond, Part 2: Recommendations for Missions

This revised white paper lists our recommendations for mission concepts and instruments to accomplish the science objectives for future exploration of Jupiter''s moon Io for the decade of 2013-2022 and beyond. (Final version with additional coauthors).

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Future Io Exploration for 2013-2022 and Beyond, Part 1: Justification and Science Objectives

This white paper (revised draft) summarizes the current scientific questions regarding Jupiter''s volcanic moon Io, and the scientific objectives and measurements that need to be accomplished by future exploration. (Final version with additional coauthors).

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Exploration Strategy for the Outer Planets 2013-2022: Goals and Priorities

Outer Planets Assessment Group (OPAG) recommends that the DS support 1) the JEO and ESJM flagship, 2) Cassini Solstice Mission, and 3) Technology to permit next Outer Planets flagship to Titan/Enceladus, and assess the feasibility of 4) "small flagship" mission class and 5) a set of NF candidates.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Determination of the physical and chemical properties of planetary systems is a key scientific goal of the James Webb Space Telescope (JWST). This white paper summarizes the mission’s capabilities in our solar system and extrasolar planetary systems.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Neptune and its captured moon Triton are unexplored with modern spacecraft instrumentation. Observations of these objects are urgently needed to address planet formation and the evolution of ice giant planets, icy satellites, Kuiper Belt Objects, and the solar system itself.

Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

The Rationale for Deployment of a Long-Lived Geophysical Network on the Moon

This paper outlines the rationale establishing a global lunar geophysical network and the authorship demonstrates the broad community support for such an endeavor, both within the USA and internationally.

The discovery of lunar magnetic fields of crustal origin was a major scientific surprise of the Apollo program. Solving the enigma of lunar remanent crustal magnetization will provide fundamental insights into the thermal history of the lunar core/dynamo, mantle, and crust, and into the processes by which crustal magnetization is acquired on airless bodies - for instance, large basin-forming impacts. Determining the origin and history of lunar crustal magnetism will require the return of oriented samples...

Science from the Moon: The NASA/NLSI Lunar University Network for Astrophysics Research (LUNAR)

The Moon is a unique platform for fundamental astrophysical measurements of gravitation, the Sun, and the Universe. With the aim of providing additional perspective on the Moon as a scientific platform, this white paper describes key research projects involving astrophysics from the Moon.

The Moon''s regolith contains vast resources of helium-3, an ideal fuel for terrestrial fusion power systems. Development of plans for private sector investment in obtaining helium-3 and its by-products requires detailed definition of that isotope''s selenographic distribution.

The Moon has attracted international attention as the current focus of peaceful competition in space. This competition has long term implications for the future of liberty on Earth. If non-democratic regimes dominate exploration and settlement of the Moon, liberty will be at risk. Only the United St

Critical differences exist between scientists who observe weather and climate and those who attempt to model nature’s complexities. The modelers believe complex mathematics and broad assumptions can forecast the future of climate, Earth’s most complex system. Long-term observation is essential.

Geological exploration by experience and highly trained field geologists provides the foundation for interpretation of lunar samples in the context of the origin and evolution of the terrestrial planets. Future lunar exploration should fully utilize the best available field geologists.

he primary difficulty in accepting the computer modeled "giant impact" hypothesis for the origin of the Moon, versus independent derivation, comes from the analysis of the non-glass components of lunar pyroclastic deposits. These prove that volatile reservoirs exist in the mantle of the Moon.

This paper describes the major questions about the atmosphere of Venus and the observations required to understand it. “How Does Venus atmosphere work?” A dedicated and renewed exploration effort is required to address this fundamental question. Key questions requiring new observations include: H

As NASA prepares to return to the Moon, a clear understanding of the chemistry of lunar dust is required to set the stage for extended duration lunar surface operations. All aspects of the unique environment of the Moon—micrometeorite bombardment, UV light exposure, solar wind radiation, solar parti

This paper discusses the capability of currently available TPS and the availability of heritage carbon phenolic used on the Pioneer-Venus probes. A prime conclusion is that there are important issues regarding the availability of the TPS required for future Venus entry probes.

We show in this white paper that, with suitable instrumentation on planetary and terrestrial spacecraft, soft X-ray emission associated with the solar wind interaction with planetary neutral atoms can map out the solar wind distribution around planets, including the locations of plasma boundaries.

Major gaps in understanding Venus include how planetary-scale crustal resurfacing operated, the formation and evolution of highlands, and whether evidence of past environments is preserved. These questions can be addressed through an orbiting radar altimeter and high resolution SAR imager.

This whitepaper describes how the next generation of lunar laser ranging addresses four key gravitational science questions. In addition, we discuss the current state of retroreflector technology and describe ways in which further advances can be made in laser ranging technologies.

The Lunar Dusty Exosphere: The Extreme Case of an Inner Planetary Atmosphere

The Moon is an extreme type of atmosphere – a surface bounded exosphere – and may represent the final ‘ground state’ of any geologically dormant body. Neutral gas and dust are emitted from its surface via universal processes believed to be occurring at all near-airless bodies.

Global Distributions of Gas & Dust in the Lunar Atmosphere from Solar Infrared Absorption Measurements with a Fourier Transform Spectrometer

Global Distributions of Dust & Gas in the Lunar Atmosphere may be determined most accurately with the highly sensitive technique of measurements of Solar IR Absorptions with a Infrared Spectrometer on a Lunar Orbiter, in full compliance with the NRC goal of measurements of Global Distributions.

It is absolutely necessary and of utmost importance to conduct the proposed measurements of charging properties of individual Apollo 11-17 submicron size dust grains by UV radiation and electron impact, at the lunar thermal cycle, for developing any believable lunar dust transportation models.

We discuss our priorities for exploring the Moon''s bombardment history: (1) Test the idea of a massive impactor spike 3.8-4.0 billion years ago. (2) Anchor the early Earth-Moon impact flux curve by determining the age of South Pole-Aitken Basin. (3) Establish a precise absolute chronology.

This paper sets out some rationales for an integrated US space development platform within the UN forums . Such a platform might include for an international lunar settlement and for a related space sciences initiative into global development

Lunar Science with ARTEMIS: A Journey from the Moon’s Exosphere to its Core [version 2]

This white paper describes the planetary science objectives to be achieved by ARTEMIS, a two-spacecraft constellation en route to the Moon, and presents recommendations pertaining to future lunar science. [version 2]

This white paper describes the science priorities developed by the Venus Exploration Analysis Group, through a series of meetings with the Venus science community. The science themes for Venus are Origin and Evolution, Venus as a Terrestrial Planet, and Climate Change and the Future of Earth.

Lunar Laser Ranging studies the Moon’s internal structure and properties by tracking the variations in the orientation and tidal distortion of the Moon as a function of time. Future missions to the Moon’s surface should include new laser ranging instrumentation capable of improved range accuracy.

A landed/mobile mission to a lunar permanently shadowed region (PSR) should identify the composition, abundance, and distribution of volatiles in lunar PSRs. The next step is obtaining a detailed understanding of the transport/deposition/retention system to unravel the history of polar volatiles.

A multiple-platform mission to Venus that includes a long-duration, circumnavigating balloon-based element, two drop sondes, and an orbiter, is described that directly addresses fundamental science iissues of planetary formation/evolution, dynamics/circulation, chemistry, meteorology, and geology.

This VEXAG community white paper covers both heritage, and key enhancing and enabling technologies, which are required for future Venus exploration missions in all three mission classes. It also argues for a targeted technology development program, including a large environmental test chamber.

This paper describes the scientific rationale for locating and studying extralunar material found in lunar regolith. The extreme age and lack of weathering of lunar regolith make it a natural repository for samples from a wide range of parent bodies and across a vast span of solar system history.

Analysis of samples returned from unexplored areas of lunar volcanism such as the Gruithuisen Domes will (1) increase our knowledge of the history of the Earth-Moon system, (2) advance theories of lunar magmatic evolution and (3) provide valuable points of comparison with other terrestrial planets.

Sampling the Age Extremes of Lunar Volcanism: the Youngest and Oldest Lunar Basalts

Automated sample return missions to the youngest (Procellarum) and oldest (cryptomaria) basalts on the lunar surface will help improve our absolute chronology for the inner Solar System by providing the timing for the beginning and end of lunar basaltic volcanism.

The lunar swirls are high albedo curvilinear surface features coincident with regions of strong remanent magnetism. Investigating the lunar swirls is important to understand the Earth-Moon system, the interaction of planetary surfaces with the solar wind, and how to best explore our solar system.

Summary and Highlights of the NRC 2007 Report: The Scientific Context for the Exploration of the Moon (SCEM)

Understanding processes that have occurred on the Moon provide a framework for understanding the origin and evolution of the other terrestrial planets. The SCEM science goals and priorities remain fundamentally relevant to our understanding of the solar system and central to its exploration.

On Lunar Volatiles and Their Importance to Resource Utilization and Lunar Science

We discuss recent, compelling evidence for major lunar volatiles not necessarily found in polar permanently-shadowed crater cold traps, but originating from the deep interior. We also discuss programs underway to study lunar volatiles, which unfortunately fall far short of the NRC''s SCEM goals.

New idea and technique with carbon cycle can be applied at lunar crust origin, lunar interior and lunar double construction (surfae and underground) building at the lunar base in future from new carbon-fixing cycle.

Constraining Solar System impact history and evolution of the terrestrial planets with exploration of and samples from the Moon’s South Pole-Aitken Basin

A fundamental issue of Solar System science is determining the early history of the terrestrial planets, including giant impact bombardment and the evolution of differentiated crust. Exploration and sampling of the Moon’s South Pole–Aitken Basin can illuminate these formative planetary processes.

Basic issues of lunar dust - including recent discoveries -so fundamental they affect a wide range of lunar research and exploration must be recognised as priorities. Four Recommendations and Outcomes are given.

Ground-Based Support for Solar-System Exploration: Continuous Coverage Visible Light Imaging of Solar System Objects from a Network of Ground-Based Observatories

We propose that the needs of planetary science for event-detection and time-critical observations could be well-served by a global network of low-cost remote-controlled (or autonomous) telescopes optimized for high-resolution visible light imaging of solar system targets.

Inner Planets: Mercury, Venus, and the Moon.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.

This paper consists of the intro & observatory capabilities (ch. 1) plus the planetary science (ch. 5) portions of the SOFIA Science Vision doc pub. in 2009 as an update of the scientific case for SOFIA. D. Backman produced this extract; the original doc is authored by the SOFIA Science Team.

Inner Planets: Mercury, Venus, and the Moon.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Space weathering is the collection of physical processes acting to erode and chemically modify planetary surfaces directly exposed to space environments of planetary magnetospheres, the heliosphere, and the local interstellar environment of the solar system. Space weathering affects the physical and

Inner Planets: Mercury, Venus, and the Moon.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Dust particles emitted from atmosphereless planetary objects are samples of their surfaces. By mass analyzing these particles and tracing back their trajectories to their sources the surface composition of Mercury, planetary satellites, dusty rings sources, asteroids and comets can be obtained.

Inner Planets: Mercury, Venus, and the Moon.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

It is the purpose of this White Paper to draw attention to, and summarize, the important role that planetary exploration, and research with a comparative planetology focus, have played and should continue to play in our understanding of climate, and climate change, on Earth.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.

I would like to draw the attention of members of the Decadal Survey Committee to a rather fundamental discovery, which (I believe) will have a major impact on the Earth and Planetary Sciences in the coming years.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.

The specific requirements for time-domain solar system science are adequate sampling rates and campaign durations. The observatory must be spaceborne both to satisfy the time-domain requirements as well as to maintain access to the dynamically significant ultraviolet spectral range.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

We have posited in another white paper that all of Planetary System Science can be seen through an astrobiological lens. In this paper we present priorities for flight mission investigations derived by applying that lens to the Planetary Science flight mission program.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Astrobiology provides a lens through which all of planetary science and solar system exploration, as well as life on Earth, can be viewed. Astrobiology, like planetary science, is a systems-level science. In planetary science, one must understand connections be [CHARACTERS NOT ACCEPTED BEYOND THIS

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

NASA’s Deep Space Network (DSN) is a critical part of every NASA solar system mission, serving as the entity that ties the spacecraft back to Earth and providing data from science instruments, information for navigating across the solar system, and valuable radio link science and radar observations.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

This paper summarizes the history, evolution and current status of analysis and archiving of planetary science data. It presents goals for PDS 2010, a revised PDS, and addresses conditions needed to achieve those goals.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Is there a feature of presence of life on a macro-level? Could we say something about life on Neptune or on Halley’s Comet or on an exoplanet? Let’s consider that sign of life is an atmosphere. Let''s consider crustal planet. Whether planet has an atmosphere we may say that it is alive in geologi

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

This white paper advocates the use of balloon-borne telescopes for diffraction-limited imaging in visible wavelengths by demonstrating their technical readiness and low cost relative to space- and ground-based facilities.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Starbursts produces extragalactic cosmic rays which initiate the Sun to develop low Planetary Indices (Kp) and low Electron flux (E-flux) condition of Sun-Earth Environment which leads to snowfall on earth and some changes in other plants of the solar system

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Funding for astrodynamics research has been largely limited to the development and operations phases of missions. Early funding for astrodynamics research would produce new techniques prior to formulation of missions, which could lead to novel and exciting concepts.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Onboard science data analysis enables new spacecraft operational modes that improve science yield. It can relieve constraints on time, bandwidth and power, and respond automatically to events on short time scales. We examine applications to rover, aerobot, and orbital platforms.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Scientists utilize radio links between spacecraft and Earth or between spacecraft to examine changes in the phase/frequency, and amplitude of radio signals to investigate atmospheres and ionospheres, rings, surfaces, shapes, gravitational fields, and dynamics of solar system bodies.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

We summarize the rationale for advocating a healthy and sustained program of laboratory research in support of the geophysical exploration of planetary bodies. We address the challenges inherent to this discipline, and we suggest recommendations for the review panel''s consideration.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Planetary science in the next decade will include major spacecraft missions to inner and outer solar system targets. Interpretation of these mission observations requires knowledge of fundamental physical and chemical properties of planetary materials. Much theoretical work at present depends upon r

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

The WGLA of the AAS promotes collaboration and exchange of knowledge between astronomy and planetary sciences and the laboratory sciences (physics, chemistry, and biology). Laboratory data needs of ongoing and next generation planetary science missions are carefully evaluated and recommended.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Giant Planets: Jupiter, Saturn, Uranus, Neptune, and exoplanets, including rings and magnetic fields, but not their satellites.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Development of Capabilities and Instrumentation for Curation and Analysis of Returned Samples

The purpose of this white paper is to emphasize the importance of investments in sample curation and analytical instrument development for the full realization of the science objectives of any sample return missions in the coming decade.

Developing Sample Return Technology using the Earth''s Moon as a Testing Ground

Lowering cost and risk through development of sample return technologies that can be used on various sample return mission styles is emphasized, as is using the Moon as a testing ground for such technologies.

The Scientific Rationale for Studying Meteorites found on Other Worlds

The ongoing identification of several meteorite candidates on Mars is ushering in a new discipline in the planetary sciences. We feel that cultivating an appreciation for the potential science return represented by meteoritic specimens on Mars and the Moon may be important for the 2013-2022 decade.

The ESPA architecture used by the LCROSS mission enables two capable missions for the cost of one launch. This paper describes our approach for leveraging the capability of the new generation of EELVs to enable secondary planetary missions at well below the cost of an independently launched mission.

EM methods can sense subsurface structure from meters to a thousand kilometers. This white paper gives a tutorial on material sensitivities, exploration depths, sources, and particularly what measurements must be made for different target bodies, without specific mission endorsements.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

The Importance of a Planetary Cartography Program: Status and Recommendations for NASA 2013-2023

We describe 7 areas where greater attention should be paid to data returned from planetary missions, beyond minimum “mission success”. The alternative is duplication of efforts and greater chances for errors, thereby diminishing the cost return and scientific potential provided by planetary data.

Inner Planets: Mercury, Venus, and the Moon.
Mars: Not Phobos and Deimos.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.
Primitive Bodies: Asteroids, comets, Phobos, Deimos, Pluto/Charon and other Kuiper belt objects, meteorites, and interplanetary dust.

Lunar Occultation Observer - A Nuclear Astrophysics Mission Concept using the Moon as a Platform for Science

The Lunar Occultation Observer (LOCO) is a gamma-ray astrophysics mission concept being developed to probe the nuclear regime. Using the Moon to occult astrophysical sources as they rise and set along the lunar limb, the encoded temporal modulation will be used to image the sky and enable science.

mm-wavelength satellite to satellite occultations combined with solar occultation and thermal IR emission aerosol measurements will tightly and uniquely constrain processes to answer key open questions about the chemistry and climate of Mars.

This white paper is intended to be a consensus of many of the active members of the Mars polar science community, and is the culmination of discussions held at the 3rd International Mars Polar Energy Balance and CO2 Cycle workshop (MPEB2009) held in Seattle, WA, 21-24 July 2009.

Update: Are There Signs of Life on Mars? A Scientific Rationale for a Mars Sample-Return Campaign As The Next Step in Solar System Exploration

Update: Discussion of the scientific rationale for Mars sample return as the next step in understanding solar-system exploration and Mars astrobiology. Sample return is discussed in the context of a Mars exploration program and the fiscal reality of the Mars program.

A consensus vision of a Mars Sample Return (MSR) mission concept is presented, reflecting the integration of multiple recent community-based planning discussions. It summarizes the current state of thought regarding the science goals that would be best addressed by samples returned from Mars.

The importance of (Noachian) impact craters as windows to the sub-surface and as potential hosts of life

The paper demonstrated the research that can be done in small craters punctuating larger Noachian craters. Topics include: small craters as natural drills, impact-generated hydrothermal systems and lakes in Noachian craters, and the ecological niches created by them.

Groundbreaking Sample Return from Mars: The Next Giant Leap in Understanding the Red Planet

The purpose of this white paper is to urge consideration of a groundbreaking sample return from Mars from a previously well characterized site that requires a simple mission architecture to minimize cost and engineering risk, while gaining substantial scientific return.

Mars'' crustal magnetization is unique and enigmatic. It is pertinent to Mars science questions as diverse as the structure of the interior and the evolution of climate. To study it, we recommend 1) extending the MAVEN mission, 2) rover-mounted surface magnetometers and 3) oriented sample return.

Summary of the Mars Science Goals, Objectives, Investigations, and Priorities

This document reflects the synthesis of recent MEPAG Goals Committee activities, MEPAG Science Analysis Groups, workshops, feedback, and discussion of these topics at recent MEPAG meetings. It was prepared by the MEPAG Goals and Executive Committees with assistance of many Mars community members.

This paper explains the importance of investigating the deep interior of Mars by seismological methods. Seismometers on Mars can bring insights to questions concerning planetary structure, tectonics, mantle and core dynamics, dynamo and mantle chemistry. The technical feasibility is assessed.

Trace gases are a sensitive indicator of current martian activity, whether photochemical or biogeochemical. A Trace Gas Mission measuring atmospheric composition, circulation and state, and locating active sources would characterize this activity and its implications for climate and astrobiology.

Technology is described which is well developed and on a path for space. This technology could be used in Mars orbit to provide a global climatology of wind and relative dust as a function of location and altitude.

I heartfully indicate the support on the sample return mission from Mars, and the indispensable facilities in laboratories. Because the sample return mission is the keys of essential problems for Planetary Science.

Near-Infrared imaging spectroscopy of the surface of Mars at meter-scales to constrain the geological origin of hydrous alteration products, identify candidate sites and samples for future in-situ and sample return missions, and guide rover operations

Near-infrared imaging spectrometers capable of mapping hydrous minerals on the surface of Mars at meter-scales from orbit, as well as hypespectral NIR imagers on landed rovers not only enhance the scientific return of orbital and rover missions, but will be critical in guiding future rover operation

Tumbleweeds are lightweight, highly configurable and inexpensive wind-driven vehicles that could enable long-range surveys of the surface of Mars. Their analytical capabilities can be optimized for measurements for astrobiology or in situ resources over relatively large swaths of terrain.

Seeking Signs of Life on Mars: In Situ Investigations as Prerequisites to Sample Return Missions

We argue for deployment of increasingly sophisticated in situ techniques to definitively identify biomarkers before engaging in Mars Sample Return. We focus on “following the nitrogen,” using techniques such as micro capillary electrophoresis to identify and determine the chirality of primary amines

Global information on martian near-surface features and physical properties represents a great untapped aspect of the search for habitable zones and evidence of past climate. Imaging radar measurements can penetrate several meters of mantling material and 10’s of meters into ice.

A process for identifying candidate landing sites for future missions should be started and accompanied by creation of funding to support landing site characterization activities. NASA should provide resources to existing missions to enable these activities and consider including instruments for sit

The Value of Landed Meteorological Investigations on Mars: The Next Advance for Climate Science

Major advances in the understanding of the present and past Mars climate system are most likely to be accomplished by in situ meteorological surface measurements operating from both a network configuration and individual stations.

Mars Exploration 2016-2032: Rationale and Principles for a Strategic Program

The Mars Exploration Program, one of the most visible and dynamic elements of NASA space science, is at a crossroads. To ensure a robust future it must embrace the related goals of life and sample return, and must begin to bridge the historical gap between robotic and human exploration.

This white paper describes a potential rover mission to Mars, with the name Mars Astrobiology Explorer-Cacher (MAX-C) that could be launched in 2018. The mission would conduct high-priority in situ science and make concrete steps towards the potential future return of martian samples to Earth.

This white paper focuses on enabling technologies for several candidate concepts for future Mars missions. These missions are described in MEPAG position white papers developed for the decadal survey. The technologies, their current status, and their approximate costs and schedules are described.

Martian soil is a microcosm of the mineralogical history of the planet, and it exerts a primary influence on atmospheric, geological, and periglacial properties. We propose an increased emphasis on microanalysis in future Mars surface exploration.

Next Steps in Mars Polar Science: In Situ Subsurface Exploration of the North Polar Layered Deposits

The polar regions of Mars represent a unique environment for determining the mechanisms of martian climate change over geological time. Using terrestrial paleoclimatology methods, subsurface access to the polar layer deposits should be a high priority for future Mars exploration.

This paper addresses the exploration of the martian atmosphere, and focuses on broad atmospheric science goals that can be obtained from orbit. It presents the key questions in atmospheric science that remain unanswered, and what progress can be made towards answering them in the coming decade.

Paper describes how a single launch Mars Sample Return (MSR) mission could potentially be enabled by using of Electric Propulsion with Hall Thrusters: a well established, off-the-shelf technology commonly used on communications satellites today.

We advocate the placement of a geophysical network on Mars to investigate the deep interior using seismic, heat flow, precision tracking and electromagnetic sounding measurements. These stations should also support meteorological atmospheric boundary layer experiments.

We present arguments for geochronology as a high scientific priority for Mars exploration in specific and planetary science in general. We also recommend funding four specific activities toward achieving technical readiness for addressing this priority.

This white paper describes the role that orbital relay telecommunications have played as an integral part of science investigation of Mars, and the importance and continuing evolution for support to future missions.

Laboratory Measurements in Support of Present and Future Missions to Mars

The case is made that supporting laboratory measurements and facilities should be considered an integral element of the Nation’s Mars exploration program, since they provide a meaningful interpretation of the returned data, validation of theoretical models, and calibration of instruments.

The ionosphere of Mars is a key part of the boundary between Mars and the solar wind. The MAVEN mission will improve our understanding of ionospheric properties and processes, including how they affect the escape to space of atmospheric species, but other important questions will remain unanswered.

Mars has been an extremely compelling exploration target. The Decadal Survey is re-evaluating the priority of different sectors of the planetary exploration program. Based on the data collected since 2002, our conclusion is that the exploration of Mars is even more compelling now than it was then.

Seeking Signs of Life on a Terrestrial Planet: An Integrated Strategy for the Next Decade of Mars Exploration

We propose an integrated strategy to implement missions of high scientific priority, as recommended by the last decadal survey, while still responding to new discoveries. The proposed step-by-step approach to sample return would provide a credible path and conduct important in situ science.

The CSNR is designing an instrumented platform that can acquire detailed data at hundreds of locations during its 10 year lifetime - a Mars Hopper. By accumulating thermal power from a radioisotope source, the platform will be able to “hop” from one location to the next every 2-3 days with a separa

Mars: Not Phobos and Deimos.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Planetary Science & Astrobiology: Cold habitats for life in the Solar system

The paper highlights that improved knowledge of the carbon and energy transformations necessary to support life at sub-zero temperatures is key to future planetary science and astrobiological research given ice is the most abundant phase of water in the Solar system.

Mars: Not Phobos and Deimos.
Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

This paper describes currently available TPS technologies and identifies new technologies needed to support Mars missions in the 2013 - 2022 timeframe, drawing on past mission studies, recent Mars Technology workshop for Mars Sample Return Mission, and the Solar System Exploration road map.

Mars: Not Phobos and Deimos.Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Solar System Suborbital Research: A Vital Investment in the Scientific Techniques, Technology, and Investigators of Space Exploration in the 21st Century.

Recent calls for increased NASA technology and training development cite shortages with current trends. Suborbital and Explorer missions are key this but have been cut in the past 20 years. Planetary research supports no small missions at all. We describe how suborbital research can address this gap

Sociological Considerations for the Success of Planetary Exploration Missions

Alongside scientific and technical considerations, the Planetary Science Decadal Survey should require that missions incorporate deeper consideration of the social science of spacecraft operations to maximize their missions’ scientific, technical and fiscal success.

Life on Earth Came From Other Planets, reviews the evidence presented in over 100 peer reviewed scientific papers published in prestigious scientific journals, and explains how life on Earth originated on other planets. The entire 45 page paper will be published in the journal, Cosmology, on 12/2009

If life were to appear on a desert island we wouldn''t claim it was assembled in an organic soup or created by God; we''d conclude it washed to shore or fell from the sky. The Earth too, is an island, orbiting in a sea of space and this is how life on our planet began.

To pursue a better understanding of life in space and link it to future missions we propose a strategy aimed at determining the potential for terrestrial microbial life to adapt and evolve in space environments. This strategy involves ground-based research, small satellite missions and will culminat

Study of primitive asteroids is fundamental to understanding the origin, distribution, and evolution of volatile and organic compounds in the early Solar System. This paper outlines six major research focus areas and recommends three mission concepts, which are listed in priority order.

Whipple: Exploring the Solar System beyond Neptune Using a Survey for Occultations of Bright Stars

Whipple is a Discovery class mission to explore the outer Solar System. A small telescope will compile lightcurves of ~40,000 stars sampled at 40 Hz. Small bodies from the Kuiper Belt to the Oort Cloud will occult targeted stars, revealing their distances, sizes, and abundances.

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Asteroids. This paper was organized by the Small Bodies Assessment Group.

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Interplanetary Dust. This paper was organized by the Small Bodies Assessment Group.

This paper presents a proposed flyby mission for one Trojan and one Centaur as designed by the participants of the JPL Planetary Science Summer School. This mission meets the current New Horizons guidelines and will address fundamental questions about the history of the solar system.

The Case for Ceres: Report to the Planetary Science Decadal Survey Committee

We present recent findings about Ceres, stressing its unique nature. Outstanding remaining science questions are discussed along with recommendations for the next steps in Ceres research in the Dawn and post-Dawn era.

Small Bodies Community White Paper: Goals and Priorities for the Study of Comets in the Next Decade (2011-2020)

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Comets. This paper was organized by the Small Bodies Assessment Group.

This white paper makes the case for sample return from primitive asteroids and comets in the next decade to address some of the most important questions in planetary science relating to the origin and history (and particularly the origin and distribution of organics and water) of the Solar System.

Small Bodies Community White Paper: Exploration Strategy for the Ice Dwarf Planets 2013-2022

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Dwarf Planets. This paper was organized by the Small Bodies Assessment Group.

This paper describes the scientific goals and implementation design of the Comet Coma Rendezvous and Sample Return (CCRSR) mission, one of the concept study missions funded by the recent NASA DSCME Program.

Currently available TPS materials can meet the needs of Sample Return missions with entry velocity <13 km/s. For entry velocity >13 km/s, heritage carbon phenolic is fully capable, but potentially unavailable and currently available TPS will need to be qualified.

NASA has examined the feasibility of sending the Orion Crew Exploration Vehicle to near-Earth objects during the next decade and beyond as part of its future Human Space Flight program. This paper describes the in-depth scientific investigations that could be accomplished by such missions.

We have no direct data on the interior structure of primitive bodies. The interior structure of asteroids is relevant to most solar system formation and evolution theories. Seismology is the only method for determining the interior structure for a range of sizes of asteroids to address.

We urge the Decadal Survey Committee, which is charged with developing “a comprehensive science and mission strategy for planetary science,” to temporarily shift research priorities in the United States from space exploration science to space utilization science.

Understanding the Saturn system has been greatly enhanced by the Cassini-Huygens mission. The proposed 7-year Cassini Solstice Mission would address new questions that have arisen during the mission, and observe seasonal and temporal change in the Saturn system to prepare for future missions.

A sizable fraction of small bodies is found in binary or multiple systems. Understanding the formation processes of such systems is critical to understanding collisional and dynamical evolution. Missions can offer enhanced science return if they target binaries or multiples. [FINAL version]

Mars'' two moons, Phobos and Deimos, are D-type small bodies that may be remnants of the population that delivered volatiles to the inner solar system. A Discovery class mission can address key science questions at the moons, and prepare for future human exploration.

The Trojan asteroids of Jupiter lie at the crux of several of the most interesting outstanding issues regarding the formation and evolution of the Solar System. We present science questions centering on the Trojans are lay out recommendations for their future study and exploration.

Small Bodies Community White Paper: The Small Satellites of the Solar System

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Small Satellites. This paper was organized by the Small Bodies Assessment Group.

Radar astrometry reduces trajectory uncertainties by orders of magnitude, thereby improving prediction, targeting, and impact probability estimates for small-bodies, while characterizing some at levels comparable to a spacecraft flyby. This improves resource use for ground and flight investigations.

Argo is an innovative pragmatic concept for a New Frontiers 4 mission which exploits an upcoming launch window that permits a close Triton encounter during a flyby through the Neptune system, and then continues on to a scientifically-selected Kuiper Belt Object.

Small Bodies Community White Paper: Goals and Priorities for the Study of Centaurs and Trans-Neptunian Objects in the Next Decade

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Centaurs and Small Irregular TNOs. This paper was organized by the Small Bodies Assessment Group.

A technology assessment and feasibility study is being performed within the ESA Advanced Concepts Team on sending a small-to-medium (700-900 kg) Nuclear Electric Propulsion spacecraft into orbit around Pluto with a mission launch in 2016 using existing or emerging space technology.

This paper identifies the top-level science issues, mission priorities, research and technology needs, and programmatic balance for the exploration of Near-Earth Objects. This paper was organized by the Small Bodies Assessment Group.

By conducting a series of piloted Near-Earth Object (NEO) missions beginning about 2020, the U.S. will reinforce the scientific, economic, programmatic, operations, planetary defense, and public outreach elements of its human exploration program.

NEO Survey: An Efficient Search for Near-Earth Objects by an IR Observatory in a Venus like Orbit

We present a conceptual design based on high-heritage flight systems from the Spitzer Space Telescope and the Kepler mission which will find 90% of all 140-meter NEOS in 7 years after launch, and by 2020, if started soon.

Imaging of asteroids is necessary to understand their physical structure for studies of solar system formation, impact hazard, and resources for exploration. Ground based imaging is required to study the population of asteroids. Radar imaging at Arecibo and Goldstone currently best achieve this task

An overview of the phenomenon, commonly dubbed the Pioneer anomaly, is given and the possibility for an experimental test of the anomaly as a secondary goal of an upcoming space mission is discussed using a putative Pluto Orbiter Probe as a paradigm.

Nobel Prize in Physics and Chemistry Could Be Awarded to Almost Anyone Who Has Done Any work In fields Including me

Almost anyone with work in chemistry and physics could be awarded the Nobel Prize; me too. Many contributions in chemistry and physics go on for several pages. The work of many are not recognized when the award is given to 1 or 2 people. Award could be given to any finding, article or discovery.

Some Anthropology of Humans in Space. Can Human Stability Provide Some Support for Non-Evolutionary or Religious Concepts? Are we able to Speak of a Homo-Astronomicus or a Human Group Involved in Space Travel? What Happens to Humans in Space? (ID-0135)

Some anthropology of humans and space. I propose a relationship between religious artifacts and astronomical stability. I establish why calling humans in space a new species fits current species understandings and mention 2 other groups-slavery and sending objects a distance. Space effects raised.

Herein we examine the atmospheric parallels between the Earth and Titan including the possibility of dramatic climate change. In the next decade, we urge extending the duration of the Cassini mission, planning for a future mission focused on Titan’s climate and other measures.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

In this white paper, we will summarize one possible mission concept to explore Enceladus within a New Frontiers-level mission: to stay below the cost cap of $650M (FY09 dollars) and within the launch capability of the Atlas V 551. We imagine that there are other possible mission scenarios...

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Due to budget constraints, the proposed Europa Jupiter System Mission is unlikely to occur as planned. We propose to split EJSM into three small, more affordable and less risky missions that return science earlier (about the same time as the launch date of ELSM) and in easier to accomodate budgets.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

With so many opportunities in the Solar System it may be hard to choose destinations. Titan has a one quality that sets it apart: it is uniquely suitable for humans. One reason for robotic Mars exploration is that humans will arrive in due course. An identical justification applies to exploring Titan

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Many of the questions remaining to be addressed after the Cassini-Huygens mission require both remote and in situ exploration. Our understanding of the lower atmosphere, surface and interior of Titan will benefit greatly from detailed investigations by a montgolfiere, reaching a variety of locations

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Europa''s icy surface may hide an ocean of liquid water. We summarize the unanswered questions pertaining to Europa following the Galileo mission, and address how those questions will be answered by suggested missions such as EJSM and a lander, as well as new telescopic and laboratory measurements.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Cassini measurements reveal that organic molecules with molecular weights of hundreds of amu are formed by photochemistry in Titan''s upper atmosphere. Investigating this chemistry is important for understanding the production of biological building blocks by naturally occurring processes.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

The outer solar system provides a rewarding assortment of planetary diversity of high interest to astrobiology. This White Paper for the 2009-2011 Planetary Science Decadal Survey evaluates the planetary bodies in the outer solar system and their value to the search for life and astrobiology.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Titan, the haze-enshrouded moon of Saturn, has the largest accessible inventory of organic molecules in the Solar System outside of the Earth. The prospects are high for the formation of prebiotic compounds not unlike what might have preceded the origin of life in the early history of the Earth.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

This White Paper describes the concept for a Titan Lake Probe, which could be implemented either as an element of a TSSM-type mission or as a stand-alone New Frontiers mission. The Lake Probe could be configured either as a boat or, for increased science return, as a submersible.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Argo is an innovative pragmatic concept for a New Frontiers 4 mission to significantly expand our knowledge of the outer Solar System. It exploits an upcoming launch window that permits a close Triton encounter during a flyby through the Neptune system, and then continues on to a scientifically-sel

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

One of the most significant discoveries made by the Cassini Mission was finding water ice particles containing organic compounds in the plume emanating from the south pole of Enceladus. Several theories for the origin of life on Earth would also apply to Enceladus. Therefore, it should be of utmos

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

Notes the science value of a network of small inexpensive landers focussed on Titan geophysics and that if appropriate radioisotope sources are available, this mission could be affordable under New Frontiers.

Satellites: Galilean satellites, Titan, and the other satellites of the giant planets.

A comprehensive strategy for Solar System exploration must identify processes common to icy worlds. Such an approach requires continued investment in discovery focused on icy satellites in the size regime 100 km and larger. We elaborate on this concept, giving specific examples and recommendations

Recommended Laboratory Studies in Support of Planetary Science: Surface Chemistry of Icy Bodies

We identify several areas where an increased emphasis on laboratory activities would lead to a significant return in scientific results, based on an enhanced understanding of the fundamental surface chemistry of icy bodies.

New Opportunities for Outer Solar System Science using Radioisotope Electric Propulsion

This whitepaper discusses how mobility provided by radioisotope electric propulsion (REP) opens up entirely new science opportunities for robotic missions to distant primitive bodies. We also give an overview of REP technology developments and the required next steps to realize REP.

These documents have been prepared in coordination with the National Academies of Science in support of the National Academies Planetary Science Decadal Survey. These documents are being made available for information purposes only, and any views and opinions expressed herein do not necessarily state or reflect those of NASA, JPL, or the California Institute of Technology.